[1]} also find that SNe Ia with early flux excess originate from younger stellar populations. This, and the early flux excess in some super-Chandrasekhar SNe Ia (e.g., SN 2020hvf; [2]}), might suggest that some early flux excess SNe Ia come from the CD scenario. The CD scenario can account for super-Chandrasekhar SNe Ia and can explain a short CEE to explosion delay time (\(t_{\rm CEED}\) ; [3]}). Therefore, it is possible that the CD scenario might account for early flux excess in some SNe Ia, but not by LTP/VLTP. Either the early flux excess results from ejecta-CSM collision like in other SN Ia scenarios (e.g., [4]}, [5]}, [6]}, [7]}), or the explosion mixes \(^{56}\) Ni to the outer regions of the SN ejecta as in some other SN Ia scenarios (e.g., [7]}, [9]}). The CSM might be gas from the planetary nebula that falls back towards the remnant. The fallback process requires further study.
